Open AccessGravitational signals due to tidal interactions between white dwarfs and black holes
Author(s) -
Casalvieri C.,
Ferrari V.,
Stavridis A.
Publication year - 2006
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2005.09773.x
Subject(s) - physics , astrophysics , white dwarf , black hole (networking) , radius , tidal heating , astronomy , orbit (dynamics) , tidal force , amplitude , gravitation , circular orbit , orbital decay , orbital elements , stars , satellite , quantum mechanics , computer network , routing protocol , routing (electronic design automation) , computer security , planet , computer science , engineering , link state routing protocol , aerospace engineering
In this paper, we compute the gravitational signal emitted when a white dwarf moves around a black hole on a closed or open orbit using the affine‐model approach. We compare the orbital and the tidal contributions to the signal, assuming that the star moves in a safe region where, although very close to the black hole, the strength of the tidal interaction is insufficient to provoke the stellar disruption. We show that for all considered orbits the tidal signal presents sharp peaks corresponding to the excitation of the non‐radial oscillation modes of the star, the amplitude of which depends on how deep the star penetrates the black hole tidal radius and on the type of orbit. Further structure is added to the emitted signal by the coupling between the orbital and the tidal motions.